Clustering properties of g-selected galaxies at z ~ 0.8

Ginevra Favole, Johan Comparat, Francisco Prada, Gustavo Yepes, Eric Jullo, Anna Niemiec, Jean Paul Kneib, Sergio A.R. Rodríguez-Torres, Anatoly Klypin, Ramin A. Skibba, Cameron K. McBride, Daniel J. Eisenstein, David J. Schlegel, Sebastín E. Nuza, Chia Hsun Chuang, Timotheé Delubac, Christophe Yèche, Donald P. Schneider

Research output: Contribution to journalArticlepeer-review

47 Scopus citations


Current and future large redshift surveys, as the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey (SDSS-IV/eBOSS) or the Dark Energy Spectroscopic Instrument (DESI), will use emission-line galaxies (ELGs) to probe cosmological models by mapping the large-scale structure of the Universe in the redshift range 0.6 < z < 1.7. With current data, we explore the halo-galaxy connection by measuring three clustering properties of g-selected ELGs as matter tracers in the redshift range 0.6 < z < 1: (i) the redshift-space two-point correlation function using spectroscopic redshifts from the BOSS ELG sample and VIPERS; (ii) the angular two-point correlation function on the footprint of the CFHT-LS; (iii) the galaxy-galaxy lensing signal around the ELGs using the CFHTLenS. We interpret these observations by mapping them on to the latest high-resolution MultiDark Planck N-body simulation, using a novel (Sub)Halo-Abundance Matching technique that accounts for the ELG incompleteness. ELGs at z ~ 0.8 live in haloes of (1 ± 0.5) × 1012 h-1M⊙ and 22.5 ± 2.5 per cent of them are satellites belonging to a larger halo. The halo occupation distribution of ELGs indicates that we are sampling the galaxies in which stars form in the most efficient way, according to their stellar-to-halo mass ratio.

Original languageEnglish (US)
Pages (from-to)3421-3431
Number of pages11
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
StatePublished - Oct 1 2016

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


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